What's New

• The Ursa Major Cluster of Galaxies. I. Cluster Definition and Photometric Data.
  • R. Brent Tully, Marc A.W. Verheijen, Michael J. Pierce, Jia-Sheng Huang, and Richard J. Wainscoat
  • 1996, Astron. J., 112, 2471.
  • Full Text in journal

• The Ursa Major Cluster of Galaxies. II. Bimodality of the Distribution of Central Surface Brightnesses?
  • R. Brent Tully and Marc A.W. Verheijen
  • 1997, Astrophys. J., 484, 145.
  • Full Text in journal

• Global Extinction in Spiral Galaxies.
  • R. Brent Tully, M.J. Pierce, J.S. Huang, W. Saunders, M.A.W. Verheijen, and P.L. Witchalls
  • 1998, Astron. J., 115, 2264.
  • Full Text in journal

• Distances from the Correlation Between Galaxy Luminosities and Rotation Rates
  • R. Brent Tully
  • Invited Chapter in `Post-Hipparcos Cosmic Candles', Eds, A. Heck and F. Caputo (Kluwer), 1999, pp. 203-223
  • preprint (astro-ph/9809394)

• Distances to Galaxies from the Correlation Between Luminosities and Linewidths. III. Cluster Template and Global Measurements of H0.
  • R. Brent Tully and Michael J. Pierce
  • 2000, Astrophys. J., 533, 744.
  • Full Text in journal

• The HI mass function in Ursa Major.
  • Marc Verheijen, Neil Trentham, R. Brent Tully, and Martin Zwaan
  • Mapping the Hidden Universe, Guanajuato, Mexico, February, 2000.
  • preprint (astro-ph/0006122)

• Radial and Transverse Velocities of Nearby Galaxies.
  • P.J.E. Peebles, S.D. Phelps, E.J. Shaya, and R. Brent Tully
  • 2001, Astrophys. J., 554, 104.
  • Full Text in journal

• The Ursa Major Cluster of Galaxies. III. Optical Observations of Dwarf Galaxies and the Luminosity Function down to M_R=-11.
  • Neil Trentham, R. Brent Tully, and Marc Verheijen
  • 2001, Monthly Notices Roy. Astron. Soc. 325, 385.
  • Full Text in journal

• Squelched Galaxies and Dark Halos.
  • R. Brent Tully, Rachel Somerville, Neil Trentham, and Marc Verheijen
  • 2002, Astrophys. J., 569, 573.
  • Full Text in journal

• The Faint End of the Galaxy Luminosity Function.
  • Neil Trentham and R. Brent Tully
  • 2002, Monthly Notices Roy. Astron. Soc. 335, 712.
  • Full Text in journal

• The NGC 5846 Group: Dynamics and the Luminosity Function to M_R=-12.
  • Andisheh Mahdavi, Neil Trentham, and R. Brent Tully
  • 2005, Astronomical J., 130, 1502.
  • Full Text in journal

• Light to Mass Variations with Environment.
  • R. Brent Tully
  • 2005, Astrophys. J., 618, 214.
  • Full Text in journal

• The Cosmological Mean Density and Its Local Variations Probed by Peculiar Velocities.
  • Roya Mohayaee and R. Brent Tully
  • 2005, Astrophys. J., 635, L113.
  • Full Text in journal

• Dwarf Galaxies in the Dynamically Evolved NGC 1407 Group.
  • Neil Trentham, R. Brent Tully, and Andisheh Mahdavi
  • 2006, Monthly Notices Roy. Astron. Soc. 369, 1375.
  • Full Text in journal

• Associations of Dwarf Galaxies.
  • R. Brent Tully, L. Rizzi, A.E. Dolphin, I.D. Karachentsev, V.E. Karachentseva, D.I. Makarov, L. Makarova, S. Sakai, E.J. Shaya
  • 2006, Astronomical J., 132, 729.
  • Full Text in journal

• Tip of the Red Giant Branch Distances. I. Optimization of a Maximum Likelihood Algorithm.
  • D. Makarov, L. Makarova, L. Rizzi, R.B. Tully, A.E. Dolphin, S. Sakai, E.J. Shaya
  • 2006, Astronomical J., 132, 2729.
  • Full Text in journal

• Tip of the Red Giant Branch Distances. II. Zero-Point Calibration.
  • L. Rizzi, R.B. Tully, D. Makarov, L. Makarova, A.E. Dolphin, S. Sakai, E.J. Shaya
  • 2007, Astrophysical J., 661, 815.
  • Full Text in journal

• The Hubble Flow around the Centaurus A/M83 Galaxy Complex.
  • Igor D. Karachentsev, R. Brent Tully, et al.
  • 2007, Astronomical J., 133, 504.
  • Full Text in journal

• Our Peculiar Motion Away from the Local Void.
  • R. Brent Tully, E.J. Shaya, I.D. Karachentsev, H.M. Courtois, D.D. Kocevskki, L. Rizzi, A. Peel
  • 2008, Astrophysical J., 676, 184.
  • Full Text in journal

• Tully-Fisher Relation.
  • R. Brent Tully, curator.
  • Tully-Fisher relation. Scholarpedia, 2(12):4485

• Midlife Crises in Dwarf Galaxies in the NGC 5353/4 Group.
  • R. Brent Tully and Neil Trentham
  • 2008, Astronomical J., 135, 1488.
  • Full Text in journal

• Discovery of New Dwarf Galaxies in the M81 Group.
  • K. Chiboucas, I.D. Karachentsev, and R. Brent Tully
  • 2009, Astronomical J., 137, 3009.
  • Full Text in journal

  

  Figure extracted from The Ursa Major Cluster of Galaxies. II.

  The panel on the left illustrates the relationship between HI line profile widths and I band absolute magnitudes for Ursa Major galaxies. Filled symbols are high surface brightness galaxies and open symbols are low surface brightness galaxies. The numbers 1,2,3 identify three high/low surface brightness pairs. The letters a,b identify two bulge/no-bulge pairs. The straight line is a regression with errors in line widths.

  The panel on the right is a plot of exponential disk central surface brightnesses and scale lengths. Symbols have the same meaning as on the left. There is sample completeness above the straight line. Note how the high/low surface brightness pairs have separated into distinct regions of the diagram.

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  • Action Principle Reconstruction of the Formation of the Local Supercluster.
    • Edward J. Shaya, R. Brent Tully, and P.J.E. Peebles
    • Oops! Never submitted.
  • Action Principle Reconstruction of the Formation of the Local Supercluster. Data and the Best Model.
    • R. Brent Tully, Edward J. Shaya, Michael J. Pierce, and P.J.E. Peebles
    • Oops! Never submitted.
  

  Figures intended for stillborn article.

  The two panels compare analyses of an N-body simulation and real data. There are two basic free parameters in the Least Action studies; mass, plotted on the vertical axis, and age of the universe, plotted on the horizontal axis. With a mass-age choice, the modeling produces distances for all the components. A chi-square evaluator is formed by comparing model and observed distances. These figures are maps of the chi-square parameter. The heavy contours are at 2 sigma significance. The vertical scales are normalized so that the tops of the panels correspond to a closed universe.

  The top panel is the chi-square map for a CDM Omega=1 N-body simulation. There is softening of the force law on scales below 250 km/s to mimic the effect of extended mass about condensations and interpenetrating halos. Ho=50 in this simulation.

  The bottom panel is the chi-square map for the Local Supercluster. The force law is softened on scales less than 300 km/s. Ho=85 is consistent with the modeling although the horizontal scale can be shifted by revision of the distance scale zero-point. The main conclusion is that the Local Supercluster is NOT well represented by a standard CDM model. Preliminary indications are that models with halos extending effectively to 400 km/s give the best fits, with Omega approximately 0.25.

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  R. Brent Tully (tully@ifa.hawaii.edu)